Mapping the temperature of the hot plasma within galaxy clusters from the spectroscopic information embedded in X-ray data has enabled tremendous advances in the understanding of merger dynamics, sloshing, and AGN feedback at low redshift [1]}, [2]}, [3]}. However, producing such temperature maps is currently unfeasible for most clusters at \(z > 0.5\)  because of the limited effective area of current X-ray observatories. Unfortunately, the next generation of X-ray observatories such as Athena and Lynx will not be operational until the 2030s. In the meantime it is essential to push the investigation of ICM dynamics and thermodynamic properties to higher redshift in order to understand how galaxy clusters formed and evolved. Fortunately, during the last decade, we have witnessed the arrival of instruments capable of mapping the SZ effect at high angular resolution on scales of few arcmin [4]}, [5]}, [6]}. The amplitude of the SZ signal being redshift independent and proportional to the ICM pressure content, the joint analysis of SZ and X-ray data offers a powerful way of mapping the ICM temperature distribution at high redshift [7]}, [8]}. Another challenging method that enables mapping the ICM temperature at high redshift consist in detecting the relativistic corrections to the SZ effect (rSZ). This method has the advantage of being independent of X-ray observations. It could therefore allow us to unveil potential calibration biases affecting the temperature measurements realized with current X-ray observatories. In this paper, we present preliminary results from two on-going programs using respectively joint analyses of X-ray and SZ data and the detection of the rSZ effect in order to map the ICM temperature of high redshift clusters.
